An ATCA radio-continuum study of the Small Magellanic Cloud - IV. A multifrequency analysis of the N 66 region

Reid, Warren A.; Payne, Jeffrey L.; Filipović, Miroslav; Danforth, Charles W.; Jones, P. A.; White, Graeme L.

doi:10.1111/j.1365-2966.2006.10017.x

Cited by 25 publications

(31 citation statements)

References 45 publications

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“…In principle, it is possible that r gd could vary significantly, in particular in the vicinity of high-mass star-formation sites, where dust destruction can become important due to supernovae explosions. Reid et al (2006) have studied the supernovae remnants within the large environment of NGC 346. These authors show that the region we study here appears largely unaffected by the impact of supernovae.…”

Section: Conversion Of Dust Surface Density To Gas Surface Densitymentioning

confidence: 99%

Star formation rates from young-star counts and the structure of the ISM across the NGC 346/N66 complex in the SMC★

Hony¹,

Gouliermis²,

Galliano³

et al. 2015

Monthly Notices of the Royal Astronomical Society

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The rate at which interstellar gas is converted into stars, and its dependence on environment, is one of the pillars on which our understanding of the visible Universe is build. We present a comparison of the surface density of young stars (Σ ) and dust surface density (Σ dust ) across NGC 346 (N66) in 115 independent pixels of 6×6 pc 2 . We find a correlation between Σ and Σ dust with a considerable scatter. A power law fit to the data yields a steep relation with an exponent of 2.6±0.2. We convert Σ dust to gas surface density (Σ gas ) and Σ to star formation rate (SFR) surface densities (Σ SFR ), using simple assumptions for the gas-to-dust mass ratio and the duration of star formation. The derived total SFR (4±1·10 −3 M yr −1 ) is consistent with SFR estimated from the H α emission integrated over the H α nebula. On small scales the Σ SFR derived using H α systematically underestimates the count-based Σ SFR , by up to a factor of 10. This is due to ionizing photons escaping the area, where the stars are counted. We find that individual 36 pc 2 pixels fall systematically above integrated disc-galaxies in the Schmidt-Kennicutt diagram by on average a factor of ∼7. The NGC 346 average SFR over a larger area (90 pc radius) lies closer to the relation but remains high by a factor of ∼3. The fraction of the total mass (gas plus young stars) locked in young stars is systematically high (∼10 per cent) within the central 15 pc and systematically lower outside (2 per cent), which we interpret as variations in star formation efficiency. The inner 15 pc is dominated by young stars belonging to a centrally condensed cluster, while the outer parts are dominated by a dispersed population. Therefore, the observed trend could reflect a change of star formation efficiency between clustered and non-clustered star-formation.

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Section: Conversion Of Dust Surface Density To Gas Surface Densitymentioning

confidence: 99%

Star formation rates from young-star counts and the structure of the ISM across the NGC 346/N66 complex in the SMC★

Hony¹,

Gouliermis²,

Galliano³

et al. 2015

Monthly Notices of the Royal Astronomical Society

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“…In particular, Gouliermis et al (2008) argue that the entire N66 region may host younger star formation events induced from the east, where the SNR B0057-724 lies (Reid et al 2006;Nazé et al 2002;Danforth et al 2003;Nazé et al 2004). There is indeed a large H i hole there, which is offset from the central parts of N66, and interesting enough, N66A lies on the triggered formation arc suggested to be associated with a shock wave coming from the direction of the SNR (their Fig.…”

Section: Discussionmentioning

confidence: 99%

“…A narrow ridge can also be discerned towards the southern outer boundary of the complex. This feature is also affected by stellar shock winds, as indicated by its remarkable [S ii] emission (Reid et al 2006). Observations with the Australia Telescope Compact Array (ATCA) and Parkes Observatory at the Australia Telescope National Facility (ATNF) also detect an H i cloud ).…”

Section: Morphologymentioning

confidence: 99%

“…An age of ∼3 Myr has been estimated for NGC 346 from evolutionary models in the H-R diagram (Bouret et al 2003). HD 5980 lies behind a SNR (B0057-724, Reid et al 2006;Nazé et al 2002;Danforth et al 2003;Nazé et al 2004), which has no known optical counterpart. Compared to the Orion Nebula, N66 has an Hα luminosity almost 60 times higher (Kennicutt 1984).…”

Section: Introductionmentioning

confidence: 99%

“…More specifically, the studies have used the radio continuum (Ye et al 1991;Reid et al 2006) and the 21 cm atomic line (Staveley-Smith et al 1997;Stanimirović et al 1999), the CO line with the SEST telescope (Rubio et al 1996(Rubio et al , 2000, the infrared with both the Infrared Space Observatory and the Spitzer Space Telescope Simon et al 2007), optical spectroscopy (Massey et al 1989;Walborn et al 2000;Evans et al 2006), ultraviolet and optical spectra (Walborn et al 2000), with data from the HST spectrograph STIS, AAT, and ESO 3.6 m telescope, imaging with ACS and WFC on board HST (Nota et al 2006), Hα (e.g., Kennicutt 1984Le Coarer et al 1993;Smith et al 2000), in the UV with the International Ultraviolet Explorer (de Boer & Savage 1980) and the Far-Ultraviolet Spectroscopic Explorer (Danforth et al 2003), and in the X-rays with XMM-Newton and Chandra (Nazé et al 2002(Nazé et al , 2004.…”

Section: Introductionmentioning

confidence: 99%

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A very young component in the pre-eminent starburst region of the Small Magellanic Cloud

Heydari-Malayeri

Selier

2010

A&A

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Context. Despite extensive research on various components of the N66/NGC 346 complex, few studies have so far focused on N66A, which is a special object in the whole complex and therefore deserves scrutiny. The study of this compact H ii region and its fellow objects seems important in the framework of massive star formation in the Magellanic Clouds.Aims. We present a study of the compact H ii region N66A in the SMC pre-eminent starburst region N66/NGC 346.Methods. This analysis is based mainly on our optical ESO NTT observations, both imaging and spectroscopy, coupled with archive HST ACS data and Spitzer infrared images (IRAC 3.6, 4.5, 5.8, and 8.0 μm).Results. We derive a number of physical characteristics of the compact H ii region N66A. For the first time using spectroscopy, we present the spectral classification of the main exciting star of N66A. Its spectral features indicate that it is a main-sequence massive star of type O8. We compare this result with that based on the stellar Lyman continuum flux estimated from the ionized gas Hβ flux.The compact H ii region belongs to a rare class of H ii regions in the Magellanic Clouds, called high-excitation blobs (HEBs). We propose that N66A probably represents a very young massive star formation event in the N66 complex that has a range of ages.

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An analysis of the FIR/RADIO continuum correlation in the small Magellanic cloud

Leverenz

Filipović

2012

Astrophys Space Sci

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The local correlation between far-infrared (FIR) emission and radio-continuum (RC) emission for the Small Magellanic Cloud (SMC) is investigated over scales from 3 kpc to 0.01 kpc. Here, we report good FIR/RC correlation down to ∼15 pc. The reciprocal slope of the FIR/RC emission correlation (RC/FIR) in the SMC is shown to be greatest in the most active star forming regions with a power law slope of ∼1.14 indicating that the RC emission increases faster than the FIR emission. The slope of the other regions and the SMC are much flatter and in the range of 0.63-0.85. The slopes tend to follow the thermal fractions of the regions which range from 0.5 to 0.95. The thermal fraction of the RC emission alone can provide the expected FIR/RC correlation. The results are consistent with a common source for ultraviolet (UV) photons heating dust and Cosmic Ray electrons (CRe − s) diffusing away from the star forming regions. Since the CRe − s appear to escape the SMC so readily, the results here may not provide support for coupling between the local gas density and the magnetic field intensity.

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An ATCA radio-continuum study of the Small Magellanic Cloud - IV. A multifrequency analysis of the N 66 region

Cited by 25 publications

References 45 publications

Star formation rates from young-star counts and the structure of the ISM across the NGC 346/N66 complex in the SMC★

Star formation rates from young-star counts and the structure of the ISM across the NGC 346/N66 complex in the SMC★

A very young component in the pre-eminent starburst region of the Small Magellanic Cloud

An analysis of the FIR/RADIO continuum correlation in the small Magellanic cloud

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